Journal
PHYSICAL REVIEW LETTERS
Volume 118, Issue 5, Pages -Publisher
AMER PHYSICAL SOC
DOI: 10.1103/PhysRevLett.118.055103
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Funding
- National Science Foundation [AST-1411879]
- National Aeronautics and Space Administration Astrophysics Theory Program Grant [NNX16AB28G]
- Ambrose Monell Foundation
- Innovative and Novel Computational Impact on Theory and Experiment (INCITE) program
- Department of Energy Office of Science User Facility [DE-AC02-06CH11357]
- Division Of Astronomical Sciences
- Direct For Mathematical & Physical Scien [1411879] Funding Source: National Science Foundation
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We present results from particle-in-cell simulations of driven turbulence in magnetized, collisionless, and relativistic pair plasmas. We find that the fluctuations are consistent with the classical k(perpendicular to)(-5/3) magnetic energy spectrum at fluid scales and a steeper k(perpendicular to)(-4). spectrum at sub-Larmor scales, where k(perpendicular to) is the wave vector perpendicular to the mean field. We demonstrate the development of a nonthermal, power-law particle energy distribution f(E)similar to E-a, with an index a that decreases with increasing magnetization and increases with an increasing system size (relative to the characteristic Larmor radius). Our simulations indicate that turbulence can be a viable source of energetic particles in high-energy astrophysical systems, such as pulsar wind nebulae, if scalings asymptotically become insensitive to the system size.
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